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VLA Polarization Observation of the Radio Arc at 15 Ghz

Published online by Cambridge University Press:  23 September 2016

M. Inoue ,
E. Fomalont ,
M. Tsuboi ,
F. Yusef-Zadeh ,
M. Morris ,
H. Tabara  and
T. Kato
M. Inoue
Affiliation:
Nobeyama Radio Observatory, Minamisaku, Nagano 384-13, Japan
E. Fomalont
Affiliation:
NRAO, Charlottesville, VA 22903, USA
M. Tsuboi
Affiliation:
Nobeyama Radio Observatory, Minamisaku, Nagano 384-13, Japan
F. Yusef-Zadeh
Affiliation:
LASP, GSFC, and Northwestern University, USA
M. Morris
Affiliation:
UCLA, Los Angeles, CA 90024, USA
H. Tabara
Affiliation:
Utsunomiya University, Utsunomiya, Tochigi 321, Japan
T. Kato
Affiliation:
Utsunomiya University, Utsunomiya, Tochigi 321, Japan

Abstract

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Polarization measurements of the radio Arc were made with the VLA at 15 GHz. High frequency polarimetry made with high spatial resolution minimizes Faraday depolarization and reveals polarized filaments which correspond to the predominant filaments of the radio Arc. We notice a peculiar linear feature in the polarization map (“thorns”) which suggests the presence of a second magnetic field system. The total intensity maps show no evidence for an interaction between the two field systems, so the thorns may be foreground magnetized structures. However, if the two magnetic field systems do interact, it would allow a model in which the acceleration of relativistic particles takes place at their intersection. The accelerated particles would flow toward both ends of the radio Arc, and account for the intrinsic polarization observed along the entire length of the system. Thermal electrons responsible for the Faraday depolarization occuring at longer wavelengths may be supplied by the interaction of the streams of relativistic particles with relatively dense, ambient thermal clouds.

Type
The Arc
Information
Symposium - International Astronomical Union , Volume 136: The Galactic Center , 1989 , pp. 269 - 274
Copyright
Copyright © Kluwer 1989 

References

Inoue, M., Takahashi, T., Tabara, H., Kato, T., and Tsuboi, M. 1984, Publ. Astron. Soc. Jpn. , 36, 633.Google Scholar
Pauls, T. Downes, D., Mezger, P.G., and Churchwell, E. 1976, Astron. Ap. , 46, 407.Google Scholar
Seiradakis, J.H., Lasenby, A.N., Yusef-Zadeh, F., Wielebinski, R., and Klein, U. 1985, Nature , 317, 679.Google Scholar
Tsuboi, M., Inoue, M., Handa, T., Tabara, H., and Kato, T. 1985, Publ. Astron. Soc. Jpn. , 37, 359.Google Scholar
Tsuboi, M. Inoue, M., Handa, T., Tabara, H., Kato, T., Sofue, Y., and Kaifu, N. 1986, Astron. J. , 92, 818.Google Scholar
Yusef-Zadeh, F. 1986, PhD Thesis, Columbia University.Google Scholar
Yusef-Zadeh, F. and Morris, M. 1987, Astrophys. J. , 322, 721.CrossRefGoogle Scholar
Yusef-Zadeh, F. and Morris, M. 1988, Astrophys. J. , 329, 729.Google Scholar
Yusef-Zadeh, F., Morris, M., Slee, O.B., and Nelson, G.J. 1986, Astrophys. J. , 310, 689.CrossRefGoogle Scholar